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Article: X-ray polarimetry of the accreting pulsar GX 301-2

TitleX-ray polarimetry of the accreting pulsar GX 301-2
Authors
KeywordsMagnetic fields
Methods: observational
Polarization
Stars: neutron
X-rays: binaries
X-rays: individuals: GX 301-2
Issue Date12-Oct-2023
PublisherEDP Sciences
Citation
Astronomy & Astrophysics, 2023, v. 678 How to Cite?
AbstractThe phase- and energy-resolved polarization measurements of accreting X-ray pulsars (XRPs) allow us to test different theoretical models of their emission, and they also provide an avenue to determine the emission region geometry. We present the results of the observations of the XRP GX 301-2 performed with the Imaging X-ray Polarimetry Explorer (IXPE). A persistent XRP, GX 301-2 has one of the longest spin periods known: similar to 680 s. A massive hyper-giant companion star Wray 977 supplies mass to the neutron star via powerful stellar winds. We did not detect significant polarization in the phase-averaged data when using spectro-polarimetric analysis, with the upper limit on the polarization degree (PD) of 2.3% (99% confidence level). Using the phase-resolved spectro-polarimetric analysis, we obtained a significant detection of polarization (above 99% confidence level) in two out of nine phase bins and a marginal detection in three bins, with a PD ranging between similar to 3% and similar to 10% and a polarization angle varying in a very wide range from similar to 0 degrees to similar to 160 degrees. Using the rotating vector model, we obtained constraints on the pulsar geometry using both phase-binned and unbinned analyses, finding excellent agreement. Finally, we discuss possible reasons for a low observed polarization in GX 301-2.
Persistent Identifierhttp://hdl.handle.net/10722/340784
ISSN
2023 Impact Factor: 5.4
2023 SCImago Journal Rankings: 1.896
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorSuleimanov, VF-
dc.contributor.authorForsblom, SV-
dc.contributor.authorTsygankov, SS-
dc.contributor.authorPoutanen, J-
dc.contributor.authorDoroshenko, V-
dc.contributor.authorDoroshenko, R-
dc.contributor.authorCapitanio, F-
dc.contributor.authorDi Marco, A-
dc.contributor.authorGonzález-Caniulef, D-
dc.contributor.authorHeyl, J-
dc.contributor.authorLa Monaca, F-
dc.contributor.authorLutovinov, AA-
dc.contributor.authorMolkov, SV-
dc.contributor.authorMalacaria, C-
dc.contributor.authorMushtukov, AA-
dc.contributor.authorShtykovsky, AE-
dc.contributor.authorAgudo, I-
dc.contributor.authorAntonelli, LA-
dc.contributor.authorBachetti, M-
dc.contributor.authorBaldini, L-
dc.contributor.authorBaumgartner, WH-
dc.contributor.authorBellazzini, R-
dc.contributor.authorBianchi, S-
dc.contributor.authorBongiorno, SD-
dc.contributor.authorBonino, R-
dc.contributor.authorBrez, A-
dc.contributor.authorBucciantini, N-
dc.contributor.authorCastellano, S-
dc.contributor.authorCavazzuti, E-
dc.contributor.authorChen, CT-
dc.contributor.authorCiprini, S-
dc.contributor.authorCosta, E-
dc.contributor.authorDe Rosa, A-
dc.contributor.authorDel Monte, E-
dc.contributor.authorDi Gesu, L-
dc.contributor.authorDi Lalla, N-
dc.contributor.authorDonnarumma, I-
dc.contributor.authorDovciak, M-
dc.contributor.authorEhlert, SR-
dc.contributor.authorEnoto, T-
dc.contributor.authorEvangelista, Y-
dc.contributor.authorFabiani, S-
dc.contributor.authorFerrazzoli, R-
dc.contributor.authorGarcia, JA-
dc.contributor.authorGunji, S-
dc.contributor.authorHayashida, K-
dc.contributor.authorIwakiri, W-
dc.contributor.authorJorstad, SG-
dc.contributor.authorKaaret, P-
dc.contributor.authorKaras, V-
dc.contributor.authorKislat, F-
dc.contributor.authorKitaguchi, T-
dc.contributor.authorKolodziejczak, JJ-
dc.contributor.authorKrawczynski, H-
dc.contributor.authorLatronico, L-
dc.contributor.authorLiodakis, I-
dc.contributor.authorMaldera, S-
dc.contributor.authorManfreda, A-
dc.contributor.authorMarin, F-
dc.contributor.authorMarinucci, A-
dc.contributor.authorMarscher, AP-
dc.contributor.authorMarshall, HL-
dc.contributor.authorMassaro, F-
dc.contributor.authorMatt, G-
dc.contributor.authorMitsuishi, I-
dc.contributor.authorMizuno, T-
dc.contributor.authorMuleri, F-
dc.contributor.authorNegro, M-
dc.contributor.authorNg, CY-
dc.contributor.authorO'Dell, SL-
dc.contributor.authorOmodei, N-
dc.contributor.authorOppedisano, C-
dc.contributor.authorPapitto, A-
dc.contributor.authorPavlov, GG-
dc.contributor.authorPeirson, AL-
dc.contributor.authorPerri, M-
dc.contributor.authorPesce-Rollins, M-
dc.contributor.authorPetrucci, PO-
dc.contributor.authorPilia, M-
dc.contributor.authorPossenti, A-
dc.contributor.authorPuccetti, S-
dc.contributor.authorRamsey, BD-
dc.contributor.authorRankin, J-
dc.contributor.authorRatheesh, A-
dc.contributor.authorRoberts, OJ-
dc.contributor.authorRomani, RW-
dc.contributor.authorSgrò, C-
dc.contributor.authorSlane, P-
dc.contributor.authorSoffitta, P-
dc.contributor.authorSpandre, G-
dc.contributor.authorSwartz, DA-
dc.contributor.authorTamagawa, T-
dc.contributor.authorTavecchio, F-
dc.contributor.authorTaverna, R-
dc.contributor.authorTawara, Y-
dc.contributor.authorTennant, AF-
dc.contributor.authorThomas, NE-
dc.contributor.authorTombesi, F-
dc.contributor.authorTrois, A-
dc.contributor.authorTurolla, R-
dc.contributor.authorVink, J-
dc.contributor.authorWeisskopf, MC-
dc.contributor.authorWu, KW-
dc.contributor.authorXie, F-
dc.contributor.authorZane, S-
dc.date.accessioned2024-03-11T10:47:05Z-
dc.date.available2024-03-11T10:47:05Z-
dc.date.issued2023-10-12-
dc.identifier.citationAstronomy & Astrophysics, 2023, v. 678-
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10722/340784-
dc.description.abstractThe phase- and energy-resolved polarization measurements of accreting X-ray pulsars (XRPs) allow us to test different theoretical models of their emission, and they also provide an avenue to determine the emission region geometry. We present the results of the observations of the XRP GX 301-2 performed with the Imaging X-ray Polarimetry Explorer (IXPE). A persistent XRP, GX 301-2 has one of the longest spin periods known: similar to 680 s. A massive hyper-giant companion star Wray 977 supplies mass to the neutron star via powerful stellar winds. We did not detect significant polarization in the phase-averaged data when using spectro-polarimetric analysis, with the upper limit on the polarization degree (PD) of 2.3% (99% confidence level). Using the phase-resolved spectro-polarimetric analysis, we obtained a significant detection of polarization (above 99% confidence level) in two out of nine phase bins and a marginal detection in three bins, with a PD ranging between similar to 3% and similar to 10% and a polarization angle varying in a very wide range from similar to 0 degrees to similar to 160 degrees. Using the rotating vector model, we obtained constraints on the pulsar geometry using both phase-binned and unbinned analyses, finding excellent agreement. Finally, we discuss possible reasons for a low observed polarization in GX 301-2.-
dc.languageeng-
dc.publisherEDP Sciences-
dc.relation.ispartofAstronomy & Astrophysics-
dc.rightsThis work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.-
dc.subjectMagnetic fields-
dc.subjectMethods: observational-
dc.subjectPolarization-
dc.subjectStars: neutron-
dc.subjectX-rays: binaries-
dc.subjectX-rays: individuals: GX 301-2-
dc.titleX-ray polarimetry of the accreting pulsar GX 301-2-
dc.typeArticle-
dc.identifier.doi10.1051/0004-6361/202346994-
dc.identifier.scopuseid_2-s2.0-85178082140-
dc.identifier.volume678-
dc.identifier.eissn1432-0746-
dc.identifier.isiWOS:001100987600010-
dc.publisher.placeLES ULIS CEDEX A-
dc.identifier.issnl0004-6361-

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